The document outlines a physics lesson plan covering topics related to telescopes, stars, galaxies, and the structure and composition of stars over 24 lessons. Key topics included refracting and reflecting telescopes, star distances and brightness, galaxies, stellar composition and nuclear fusion, and how a star's color relates to its surface temperature.
This document contains a learning activity worksheet on light, reflection, refraction, and how electrons behave as waves. It includes multiple choice questions, fill-in-the-blank activities, and short answer questions to test students' understanding of key concepts. Students are asked to define terms, describe phenomena like the photoelectric effect, and explain how experiments provide evidence that electrons exhibit wave-like properties. The various activities assess students' knowledge of the wave and particle nature of light and electrons.
This document contains multiple choice questions and answers from Chapter 5 of the textbook "The Cosmic Perspective". The chapter discusses light and matter, including how light interacts with matter, the nature of light as both a wave and particle, the electromagnetic spectrum, and atomic structure and spectra. Key points covered include how light can be absorbed, transmitted, or reflected by matter, the wave-particle duality of light, and how the temperature of an object determines the peak wavelength in its thermal radiation spectrum.
This document contains a learning activity worksheet for a Grade 12 Physical Science class. It includes multiple choice questions, true/false questions, and activities about various light phenomena and the discovery of radio waves. Some of the topics covered include rainbow formation, color absorption and reflection, scattering of light in the atmosphere, mirages, halos and sundogs. It also addresses Hertz's experiments producing and detecting radio waves and how this discovery led to important applications of radio waves in areas like broadcasting and wireless communication.
This document contains a series of multiple choice questions about telescopes and astronomical observation. The questions cover topics like the basic functioning of reflecting and refracting telescopes, the advantages of larger telescope size and space-based telescopes, interferometry techniques, and common instruments attached to telescopes.
This document contains a learning activity worksheet about motion and the development of models of the universe. It includes multiple choice and fill-in-the-blank questions about Greek astronomers like Aristotle, Ptolemy, and Copernicus and their cosmological models. It also covers Galileo's ideas about motion, including that objects in motion will remain in motion unless acted upon by an external force. Students are asked to analyze experiments on falling objects in air and vacuum and distinguish between Galileo's views on horizontal motion and Newton's first law of motion.
The document is a learning activity worksheet about special and general relativity. It contains multiple choice questions, matching activities, and short answer questions about key concepts of relativity such as mass-energy equivalence, reference frames, postulates of special relativity, and consequences of general relativity like gravitational redshift and black holes. The worksheet aims to explain the consequences of the postulates of both special and general relativity.
Special relativity revolutionized our understanding of space and time by showing that they are relative rather than absolute. Key ideas include:
- No object can exceed the speed of light, and the speed of light is the same in all reference frames.
- Time passes more slowly and lengths contract for objects in motion, with dramatic effects near light speed.
- Simultaneity of events depends on one's perspective; time and space are relative rather than absolute concepts.
The document discusses the history of models of the solar system from Ptolemy's geocentric model to Copernicus' heliocentric model, which Galileo later provided evidence for using a telescope. It also describes how telescopes have improved over time and allowed for the discovery of more planets and insights into the solar system and beyond. Modern observations show there are billions of galaxies in the universe and our sun is one of millions of stars in the Milky Way galaxy.
The Sun shines through nuclear fusion in its core. The core is hot and dense enough for hydrogen to fuse into helium via the proton-proton chain reaction. This nuclear fusion releases energy that gradually makes its way to the surface and radiates into space, powering the Sun for billions of years. We know about the Sun's interior structure from mathematical models, observations of solar vibrations, and detections of solar neutrinos. Solar activity like sunspots and solar flares are caused by magnetic fields in the Sun. Bursts of particles from solar activity can disrupt power grids and satellites orbiting Earth. The 11-year solar cycle is due to changes in the Sun's magnetic field over time.
The document contains a reading quiz with multiple choice questions about telescopes and observational astronomy. It covers topics like how the eye and cameras work as light detectors, the basic designs and properties of telescopes, the effects of the atmosphere on ground-based observations, and parts of the electromagnetic spectrum that can only be observed from space. The questions are about details within these topics, such as what part of the eye is analogous to a camera's detector, the advantages of space telescopes over ground-based ones, and which part of the spectrum NASA's SOFIA observatory observes.
The document summarizes key concepts about exploring space through electromagnetic radiation and telescopes. It discusses how light from distant stars and galaxies takes years to reach Earth, and how different types of telescopes like optical and radio telescopes are used to observe electromagnetic radiation from space. Important space exploration missions and discoveries are also outlined, like the Voyager probes, Galileo probe, Apollo moon landings, the space shuttle program, and the International Space Station.
The document contains multiple choice questions and answers about key concepts regarding the Sun from Chapter 14 of The Cosmic Perspective textbook. Specifically, it addresses questions about why the Sun shines, the conditions required for nuclear fusion, how photons move from the Sun's core to its surface, the solar activity cycle, and how solar activity affects Earth.
This document summarizes a chapter about telescopes. It discusses how telescopes work by focusing light using lenses or mirrors. The two most important properties of telescopes are their light-collecting area and angular resolution. There are two basic designs: refracting telescopes use lenses while reflecting telescopes use mirrors. Astronomers use telescopes to take images, perform spectroscopy, and monitor light over time. Earth's atmosphere limits ground-based observations so many telescopes are placed in space. Telescopes observe different wavelengths of light by modifying their designs. Multiple telescopes can work together using interferometry to achieve very high angular resolution.
This document outlines the key topics and activities covered in a module on light. It begins with an introduction focusing on identifying the effects of factors on motion based on laws of motion. It then discusses the transitions between grades 3-6 and 7-10 on topics like sources and properties of light. The objectives of the current session are to relate lessons to concepts covered in the quarter and perform an activity demonstrating that white light is composed of colors that bend differently when passing through a prism. The activity involves using a prism and water to separate white light into a visible spectrum. Questions ask students to observe and explain the color arrangement and how it demonstrates the dispersion of light.
Radio astronomy is a fascinating science and it studies the Universe by detecting radio emission from many objects like the Sun, the Milky way, planets, galaxies and nebulas. In this presentation Filippo Bradaschia, PrimaLuceLab president and co-founder, gives an overview on radio astronomy history and basic physics. Then he introduces the most important radio sources in the Universe and the SPIDER affordable radio telescopes developed by PrimaLuceLab with Radio2Space brand. These instruments allow any school, university, museum or science institute to make real radio astronomy with powerful but affordable, compact and easy to use radio telescopes.
There are many ways to view the universe beyond just visible light. Telescopes collect different wavelengths of light and energy, from optical to infrared, radio, ultraviolet, x-rays, and gamma rays. Each type of telescope reveals different information and allows us to study different phenomena in the universe. The best locations for telescopes are high mountain tops for optical and infrared telescopes, and space for telescopes studying wavelengths blocked by Earth's atmosphere like x-rays and gamma rays. Advanced telescopes working together across the electromagnetic spectrum provide scientists with more complete data to understand the formation and evolution of the universe.
Edwin Hubble used the 48-inch Palomar Telescope in 1949 to make discoveries. There are three main types of telescopes: refractors which use lenses, reflectors which use mirrors, and compound telescopes which use both lenses and mirrors. The aperture and focal length of a telescope determine its light gathering ability and magnification. Atmospheric conditions like light pollution, turbulence, and temperature affect telescope views.
The James Webb Space Telescope will launch in 2018 to be the foremost space telescope of the next decade. With infrared imaging capabilities, it will see further back in time than previous telescopes to observe the formation of the first stars and galaxies as well as the evolution of planetary systems. The JWST's goals are to search for the earliest galaxies and stars, determine how galaxies evolve over time, observe star and planet formation, and examine exoplanets for potential habitability. It will accomplish these goals using a large primary mirror, instruments sensitive to infrared wavelengths, and the ability to detect highly redshifted light from the earliest objects in the universe.
The document discusses the cosmic microwave background radiation. It was discovered in 1964 by Arno Penzias and Robert Wilson, though first predicted in 1948. It represents the heat left over from the Big Bang and provides evidence that the universe was once much smaller, hotter, and denser. It is electromagnetic radiation that has freely streamed from an early epoch when the Universe became transparent for the first time to radiation.
VisMed3D-Community Mirrors and 3D Trends Shaping Our Lives in Healthcare Dima Elissa, MBA
Dima Elissa, MBA CEO and Founder of VisMed3D presents a provocative lens on the future in healthcare using 3D Printing and 3D design. The software features and capabilities in the design tools are shaping trends happening in in the world. This impacts building design and healthcare considerations inside the walls, and the pace and speed of innovation architects need to know.
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The document discusses the implementation of a Supplemental Instruction (SI) program at The Citadel School of Engineering to increase retention of engineering students. Prior to 2011, retention rates were low, with about half of freshmen leaving the major before sophomore year. In 2011, the president tasked departments with increasing enrollment by 10% by 2015. The School of Engineering implemented SI in core engineering and prerequisite courses like math, chemistry, and physics. After expanding the program, DFW rates decreased in those courses from 2012 to 2013 while increasing slightly in engineering courses, showing initial success. The challenges of training student leaders and promoting the new program were addressed through meetings and marketing.
The document summarizes the results of an activity where students identified risks and safety measures from illustrations. They analyzed 13 pictures and listed multiple risks seen in each, such as unprotected belts, heavy loads, improper ladders, exposed wiring, and more. Recommended safety measures addressed covering belts, using wheelbarrows for heavy loads, closing doors, installing handrails around holes, and more. The activity was part of commemorating World Day for Safety and Health at Work.
Ivan Petrov is a 62-year-old man from Plovdiv, Bulgaria who lives with his wife. He worked as a miner for 25 years in mines around Sofia, working long hours in difficult conditions hundreds of meters underground. Now retired at age 45 due to the physically demanding nature of his job, he receives a pension and spends time with his family in Plovdiv.
Pepe is a 48-year-old painter who owns his own painting business in Málaga, Spain. He lives with his wife and two children, Carlos and Angela, in a middle-class neighborhood. Carlos is studying to join the police force while Angela is studying travel agency courses. Pepe works long hours from 7am to 6:30pm painting buildings and infrastructure, though his income varies depending on how much work he has each month.
Alejandro Ortega Tirado is a 20-year-old lifeguard from Málaga, Spain who works at Adelfas. He earns 1,000€ per month working 10 hours per day with a temporary contract. He completed his primary and secondary education from 1997-2007 and obtained a National Electrician Diploma from 2008-2010 before becoming a lifeguard in 2011-2012. He speaks Spanish natively and English at an intermediate level.
This document provides an overview of the key concepts and lessons covered in a physics module on forces and motion. Over 12 lessons, students will learn about forces in different directions, how objects start and stop moving, friction, reaction forces, speed, modeling motion, force interactions, momentum, changes in momentum, car safety, laws of motion, work and energy, and kinetic and gravitational potential energy. Example questions and activities are provided to help students understand concepts like momentum, changes in momentum due to forces, and how safety features in cars like seatbelts reduce impact forces during collisions.
The document is a compilation of mathematics questions and answers from CIE examinations for pure mathematics 2 and 3. It was compiled by the RACSO group and contains questions on vectors and other topics across 14 pages. The questions and answers are intended to help students in their CIE examinations.
The document is a study guide for an exam on Chapter 4 about stars and the Milky Way galaxy. It contains multiple choice questions about key concepts like the Milky Way being a spiral galaxy, astronomers using parallax to measure distance to stars, convection not being how hydrogen fuses into helium, and white dwarfs being the final stage of low-mass stars. The study guide emphasizes understanding mass determining a star's life cycle and convection versus fusion as common mistakes. It provides review of class demonstrations and diagrams about stellar evolution.
Astronomy is the scientific study of celestial objects and phenomena that originate outside the Earth's atmosphere. In modern times, astronomy is defined as the science of the universe outside of Earth. Key areas of astronomy include cosmology, astrometry, planetology, and radio astronomy. Optical telescopes use lenses to collect and focus light, while radio telescopes use large concave mirrors. Other instruments like spectroscopes, photometers, and interferometers are also used. The universe originated from a massive expansion known as the Big Bang, and theories about its future evolution and structure continue to be explored. Galaxies, stars, and planetary systems are some of the main components of the universe studied by astronomers.
This document discusses methods for determining properties of stars such as their distance, luminosity, radius, and mass. It explains that trigonometric parallax can be used to measure distances to nearby stars within 50 parsecs. Absolute magnitude and distance modulus relationships allow calculation of intrinsic brightness. A star's luminosity is proportional to its radius squared, so comparing luminosities determines relative radii. The Hertzsprung-Russell diagram organizes stars by temperature and luminosity, revealing populations like giants and dwarfs. Masses can be estimated using Kepler's laws applied to binary star orbits in visual, spectroscopic, and eclipsing binary systems. Large surveys aim to characterize the diversity of stars within our galaxy.
The document summarizes information about the formation and evolution of stars, including our sun. It discusses how stars are formed from collapsing gas clouds, and how stars of different masses will evolve differently. Lower mass stars like our sun will become red giants and end as white dwarfs, while very massive stars may explode as supernovae and form neutron stars or black holes. It also provides information about classifying and identifying properties of stars using tools like spectroscopy and star charts.
The Stars of the Sky and their Life Cycles (2).pptxBricemilet
The document discusses the life cycles of stars from their birth in molecular clouds to their evolution on the main sequence and eventual death. It begins by explaining how stars are born from collapsing gas and dust in molecular clouds. It then describes how protostars form and evolve into pre-main sequence stars. Next, it discusses how stars exist on the main sequence fusing hydrogen until more massive stars die in supernovae while less massive stars become white dwarfs. The document also provides details on properties of stars like luminosity, temperature, and how the Hertzsprung-Russell diagram is used to study stellar evolution.
This document provides an overview of the characteristics, classifications, motions, and significance of stars. It discusses their sizes, colors, temperatures, compositions, and magnitudes. Stars are classified based on their spectral types, which relate to their surface temperatures. The Hertzsprung-Russell diagram plots stars' luminosities and temperatures. Stars exhibit both apparent and actual motions, including proper motion across the sky. Studying stars helps us understand how elements are formed, how our solar system evolved, and the dynamics influencing galaxies.
Materials Required· Computer and internet access· Textbook· AbramMartino96
Materials Required
· Computer and internet access
· Textbook
· Scientific calculator
· Spreadsheet software like Excel
· Digital camera
· Printer or drawing software
· Save this worksheet and use it as your report template
Time Required: Between 3-3.5 hours, note that depending if you use Excel (or similar), your time will be shortened.
Introduction
Figure 1: JP Stellar Revolution
The life cycle of the stars is one of the most fascinating studies of astronomy.Stars are the building blocks of galaxies and by looking at their age, composition and distribution we can learn a great deal about the dynamics and evolution of that galaxy. Stars manufacture the heavier elements including carbon, nitrogen and oxygen which in turn will determine the characteristics of the planetary systems that form around them. It is the mass of the star which will determine its life cycle and this all depends on the amount of matter that is available in its nebula. Each star will begin with a limited amount of hydrogen in their cores. This lifespan is proportional to (f M) / (L), where f is the fraction of the total mass of the star, M, available for nuclear burning in the core and L is the average luminosity of the star during its main sequence lifetime. The larger the mass, the shorter the lifespan ending in a beautiful supernova, the smaller the mass, the longer the lifespan ending as a quiet brown dwarf (Fig. 1).
Main Sequence Stars
Figure 2: https://imagine.gsfc.nasa.gov/
For this lab we will focus on stars similar to our own Sun (up to 1.4MassSun ), main sequence stars. A star that is similar in size to our Sun will take approximately 50 million years to mature from the beginning of their collapse to becoming an “adult” star. Our Sun, after reaching this mature phase, will stay on the main sequence of the HR-diagram for approximately 10 billion years (Fig. 2). Stars like our Sun are fueled by the nuclear fusion of hydrogen forming into helium at their cores. It is this outflow of energy that provides the outward pressure necessary to keep the star from collapsing under its own weight. And in turn, this energy determines the luminosity of the stars.
Death of Our Sun
Figure 3. NGC 6543
When a low mass star like our Sun has exhausted its supply of hydrogen in its core, then there will no longer be a source of heat to support the core against the pull of gravity. Hydrogen will continue to burn in a shell around the core and the star will evolve into the phase of a red giant, growing in diameter. The core of the star will collapse under the pull of gravity until it reaches a high enough density, and it will begin to burn helium and make carbon. This phase will last about 100 million years eventually exhausting the helium and then becoming a red supergiant, growing more in diameter. This is a more brief phase and last only a few tens of thousands of years and the star loses mass by expelling a strong wind. The star eventually loses the mass in its envelope, leav ...
Materials Required· Computer and internet access· Textbook· AbramMartino96
Materials Required
· Computer and internet access
· Textbook
· Scientific calculator
· Spreadsheet software like Excel
· Digital camera
· Printer or drawing software
· Save this worksheet and use it as your report template
Time Required: Between 3-3.5 hours, note that depending if you use Excel (or similar), your time will be shortened.
Introduction
Figure 1: JP Stellar Revolution
The life cycle of the stars is one of the most fascinating studies of astronomy.Stars are the building blocks of galaxies and by looking at their age, composition and distribution we can learn a great deal about the dynamics and evolution of that galaxy. Stars manufacture the heavier elements including carbon, nitrogen and oxygen which in turn will determine the characteristics of the planetary systems that form around them. It is the mass of the star which will determine its life cycle and this all depends on the amount of matter that is available in its nebula. Each star will begin with a limited amount of hydrogen in their cores. This lifespan is proportional to (f M) / (L), where f is the fraction of the total mass of the star, M, available for nuclear burning in the core and L is the average luminosity of the star during its main sequence lifetime. The larger the mass, the shorter the lifespan ending in a beautiful supernova, the smaller the mass, the longer the lifespan ending as a quiet brown dwarf (Fig. 1).
Main Sequence Stars
Figure 2: https://imagine.gsfc.nasa.gov/
For this lab we will focus on stars similar to our own Sun (up to 1.4MassSun ), main sequence stars. A star that is similar in size to our Sun will take approximately 50 million years to mature from the beginning of their collapse to becoming an “adult” star. Our Sun, after reaching this mature phase, will stay on the main sequence of the HR-diagram for approximately 10 billion years (Fig. 2). Stars like our Sun are fueled by the nuclear fusion of hydrogen forming into helium at their cores. It is this outflow of energy that provides the outward pressure necessary to keep the star from collapsing under its own weight. And in turn, this energy determines the luminosity of the stars.
Death of Our Sun
Figure 3. NGC 6543
When a low mass star like our Sun has exhausted its supply of hydrogen in its core, then there will no longer be a source of heat to support the core against the pull of gravity. Hydrogen will continue to burn in a shell around the core and the star will evolve into the phase of a red giant, growing in diameter. The core of the star will collapse under the pull of gravity until it reaches a high enough density, and it will begin to burn helium and make carbon. This phase will last about 100 million years eventually exhausting the helium and then becoming a red supergiant, growing more in diameter. This is a more brief phase and last only a few tens of thousands of years and the star loses mass by expelling a strong wind. The star eventually loses the mass in its envelope, leav ...
The document summarizes key concepts in astronomy, including:
- Astronomy is the study of objects outside Earth, while astrology uses celestial objects to predict events.
- Light and other electromagnetic radiation provide information about distant stars and galaxies. Spectral analysis reveals the composition of stars.
- The universe is immense, with distances measured in light years due to the finite speed of light. Stars have different properties based on size, temperature, brightness, and more.
- Stars evolve over their lifetime according to nuclear fusion processes in their cores until ending as white dwarfs, neutron stars, or black holes depending on their mass.
- Galaxies come in spiral, elliptical, and irregular forms, with the Milky Way
Chapter 10 discusses methods for measuring properties of stars, including:
1) Parallax is used to measure distances to nearby stars, with the nearest being Proxima Centauri.
2) Luminosity is a star's absolute brightness, while apparent brightness depends on distance and luminosity.
3) Spectral classes correspond to surface temperatures, ranging from hottest O stars to coolest M stars.
4) The Hertzsprung–Russell diagram plots luminosity vs temperature, showing most stars on the main sequence.
The document describes an activity using a balloon to model the expansion of the universe. Students mark dots representing galaxies on an uninflated balloon and measure the distances between them. After inflating the balloon, the distances have increased, simulating the observed expansion of space in the actual universe. The activity shows that as the space between objects expands, the wavelength of light from distant galaxies appears redshifted. While useful, the balloon model has limitations and a three-dimensional model may better represent the large-scale structure of our expanding universe.
The document discusses various topics related to stars and astronomy, including:
1) It describes the Sun and stars, and how their brightness, color, and names are determined. Distance and temperature affect a star's observed properties.
2) Precise measurements of nearby stars were made by the Hipparcos satellite in the 1990s, allowing their distances and properties to be better understood.
3) Spectroscopy is used to determine stars' chemical compositions and physical conditions by analyzing spectral lines from their emitted light.
Intro to astrophysics nis grade 11 by mr marty, visible brightness = apparent...Michael Marty
History of magnitude scales; brightness, luminosity, and Power of a star; Stefan-Boltzmann Law; Stellar Parallax; and Wien's Displacement Law of blackbody radiation.
- The document is a student's chemistry project on space chemistry. It thanks the teacher and school for allowing the project and providing resources.
- The project covers topics like the chemical composition of space, how space suits work, rocket propellants, and harnessing energy from space. It includes sections on stars and their properties, the life and death of stars, and references.
The document discusses various topics relating to stellar characteristics and evolution. It begins by explaining blackbody radiation and Wien's law, which show the relationship between an object's temperature and the wavelength of its peak emission. This allows astronomers to determine a star's surface temperature from its spectrum. The rest of the document discusses stellar classification schemes, the Hertzsprung-Russell diagram, the life cycles of different types of stars such as red giants and white dwarfs, and phenomena like supernovae, pulsars, and binary star systems. Spectral analysis provides insights into stellar physics and evolution.
This document provides an overview of stars, galaxies, and the universe. It begins with definitions of key terms like stars, galaxies, and the universe. It then covers the composition of stars and how they are classified. The next sections discuss the life cycles of stars and the different types of galaxies. The document concludes with an explanation of the big bang theory of the universe and how scientists estimate the age of the universe.
Habiatal Zone (outside our solar system)Bob Smullen
The document discusses the habitability of planets outside our solar system. It covers topics like the habitable zones around different types of stars where liquid water could exist, methods used to detect exoplanets, and factors that influence a planet's potential habitability such as size, atmosphere, and distance from the host star. It also examines probabilities for life elsewhere in the galaxy based on the Drake Equation and considers challenges around detecting and communicating with intelligent civilizations.
This document provides an overview of astronomy concepts including:
1. It describes the distances and locations of nearby stars like Proxima Centauri, Alpha Centauri, and Sirius.
2. It explains how stellar parallax can be used to measure the distances to stars, where a star with a parallax of 1 arcsecond is 1 parsec away.
3. It discusses how the brightness of stars decreases with the inverse square of their distance due to light spreading out over a greater area, known as the inverse square law.
The document provides information about stars and constellations, including defining what a star is, explaining the brightness and temperature of stars, and how stars are grouped into constellations. Key details covered include the two characteristics that define brightness, the relationship between surface temperature and color, different sizes and masses of stars, and how stars are born from nebulae. The document aims to teach readers about various properties and life cycles of stars.
T1. solar system 3, plates, orbits, periods, light,jaume2014
The document provides information about the solar system, including:
- The eight planets that orbit the sun in elliptical orbits, along with their relative sizes, masses, distances from the sun, and orbital periods.
- Other objects in the solar system like moons, asteroids, meteoroids, and comets are described.
- Concepts like reflection, light, shadows, day and night, and planetary rotation are explained. Experiments are suggested to investigate light, shadows, and reflection.
- Key data on planetary properties are presented in a table for comparison, and a graph shows the relationship between orbital distance and period.
The document outlines a route map for a 12 lesson course on electric circuits. It will cover topics like static electricity, electric charge, circuits, current, resistance, resistors, voltage, power, and electricity generation and distribution. It provides learning objectives and a sample activity for the first lesson which involves drawing a series circuit with batteries, a switch, light bulb, resistor and variable resistor and adding a voltmeter and ammeter.
This document provides an overview of the topics that will be covered in 12 lessons on electric circuits. The lessons will cover static electricity, electric charge, circuit symbols, simple circuits, controlling and measuring current, resistance, resistor combinations, measuring voltage, electrical power, domestic appliances, generating electricity, and distributing electricity. Each lesson will have objectives, activities, extension questions, and a summary.
The document outlines a 12 lesson plan on the topic of forces and motion. It will cover key concepts such as forces in different directions, how objects start to move, friction, reaction of surfaces, speed, modeling motion, force interactions, changes in momentum, car safety, and laws of motion. Each lesson will include objectives, activities, literacy and numeracy focuses, and questions to help students understand the key topics being covered.
1. The document outlines a route map for a chemistry module covering topics like alkanes, alcohols, carboxylic acids, and energy changes over 24 lessons.
2. Lesson C7.9 focuses on rates of reaction and how factors like temperature, concentration, and particle size can influence the rate. Collision theory and activation energy are also discussed.
3. Examples of reversible reactions are given where the direction can change based on conditions like temperature and pressure. Equilibrium is reached when the rates of the forward and reverse reactions are equal and concentrations no longer change.
This document outlines a chemistry lesson plan covering titrations. The lesson will teach students how titration is used as a quantitative technique to measure the concentrations of acids and bases by determining the volume needed of a standard solution to reach the endpoint of a neutralization reaction. Key concepts include using an indicator to identify the endpoint, repeating titrations to obtain an accurate average volume, and how titrations can be used to find the concentration of an unknown solution based on the reaction stoichiometry. The lesson will also discuss using data loggers and pH probes for higher precision measurements.
The document outlines a chemistry route map for studying various topics over 24 lessons, including alkanes, alcohols, carboxylic acids, esters, fats and oils, energy changes, chromatography, titrations, reaction rates, equilibrium, the chemical industry, and green chemistry. It provides lesson objectives, activities, and questions for lessons on alkanes, alcohols, and carboxylic acids, covering topics like their structures, properties, reactions, uses, and how they are produced.
This document outlines a route map for a chemistry module covering topics like alkanes, alcohols, carboxylic acids, esters, fats and oils, energy changes, chromatography, gas chromatography, titrations, rates of reaction, equilibrium, the chemical industry, green chemistry, industrial chemistry, theories on acidity, sampling, and making ethanoic acid. The module will focus on improving yield in industrial chemistry and reducing waste and pollution.
This document provides an overview of a 12-lesson chemistry module that will cover various topics related to chemical synthesis, including the chemical industry, acids and alkalis, rates of reactions, and factors that affect rates. It focuses specifically on lesson 6.11, which discusses the different stages involved in chemical synthesis, and lesson 6.12, which is about measuring the yield of chemical reactions.
The document provides an overview of a 12-lesson course on chemical synthesis that covers topics such as the chemical industry, acids and alkalis, reactions of acids, salts, purity of chemicals, rates of reactions, catalysts, chemical quantities, stages of chemical synthesis, and measuring yield. The first lesson focuses on understanding the role and importance of the chemical industry and the difference between bulk and fine chemicals.
This document outlines a lesson plan on metals from the lithosphere. It will teach students how reactive metals are extracted from ores using methods like carbon displacement and electrolysis. Key concepts include metal ores, extraction methods, reactivity series, and calculating formula masses of compounds. Activities include matching metals to their ores, naming metals, and explaining extraction techniques and material uses based on reactivity.
This document provides an overview of the lessons that will be covered in a course on chemicals in the natural environment. The 12 lessons will cover chemicals found in the atmosphere, hydrosphere, lithosphere and biosphere. It outlines the key concepts, objectives and activities for the first lesson which will introduce the four spheres and focus on the chemicals found in each.
1. Ionic compounds form when a metal reacts with a non-metal, resulting in positively charged metal ions and negatively charged non-metal ions that bond together in a crystalline lattice structure.
2. When ionic compounds dissolve in water or melt, the ions become free to move and conduct electricity. During electrolysis, positively charged metal ions move to the cathode and negatively charged non-metal ions move to the anode.
3. Common ionic compounds include sodium chloride, formed from sodium and chlorine ions, and copper chloride, used in electrolysis to extract copper metal from its ionic form.
The document provides an overview of a 12-lesson chemistry course covering topics like the periodic table, alkaline metals, chemical equations, halogens, helium, atomic structure, electrons, salts, and ionic theory. It includes lesson objectives, activities, extension questions, and summaries for the first two lessons which focus on the periodic table and alkaline metals. Key points covered are the periodic table's arrangement of elements, properties of group 1 alkaline metals like their reactions with water and acids, and their similarities and reactivity trends.
This document outlines a biology curriculum covering various topics over 12 lessons. It will cover photosynthesis, respiration, feeding relationships, genetics, blood, circulation, energy, symbiosis, parasites, disease, biotechnology, exercise, joints, genetic modification, and more. Key concepts include how plants and organisms obtain and use energy, genetic inheritance and testing, the structure and function of body systems, and applications of biotechnology.
Genetic testing uses gene probes to identify inherited disorders in embryos or fetuses. It was developed in the 1980s and can detect conditions like cystic fibrosis, sickle cell anemia, and Down syndrome. A gene probe is a piece of DNA that binds to a faulty gene, identifying disorders. Parents may choose to terminate a pregnancy if testing finds an inherited disease.
The document outlines a biology lesson plan covering photosynthesis and respiration over 12 lessons. Lesson 2 focuses on how plants trap light energy during photosynthesis. It discusses how chloroplasts in plant cells contain chlorophyll which absorbs light and uses it to split water and combine it with carbon dioxide to produce glucose and oxygen. Glucose acts as a stored form of chemical energy.
This document outlines a biology course curriculum covering various topics related to photosynthesis, respiration, circulation, genetics, and more over 12 lessons. It then provides details on one specific lesson regarding breathing and gas exchange, including objectives, key concepts, and assessment questions. The lesson focuses on how the lungs, alveoli, and blood vessels facilitate the rapid exchange of oxygen and carbon dioxide between inhaled air and blood.
This document provides an overview of the 12 lessons to be covered in the B6 module on the brain and mind. It focuses on learned behavior and conditioning. Key points covered include:
- Animals can learn new behaviors through conditioning, such as a dog salivating when it sees its food bowl.
- Pavlov's experiment showing how dogs can learn to associate a bell with being fed through repeated conditioning.
- Studies showing how an animal's response time, such as a cat escaping a trap, decreases with repeated practice and learning.
This document provides an overview of the 12 lessons that will be covered on the topics of the brain and mind. It focuses on lesson 1 which discusses what behavior is, simple reflexes in humans like newborns, and how reflexes help with survival. Newborn babies have reflexes like grasping, sucking, and stepping to help them in the first months before they are nurtured by parents. Sudden infant death syndrome has been linked to problems with reflexes in babies.
This document provides an overview of a 12-lesson module on growth and development. The lessons will cover topics like growing and changing, growth patterns, cell reproduction, genetics, specialized cells, and proteins. Key concepts include DNA, genes, inheritance, cell division, and how cells become specialized.
How to Store Data on the Odoo 17 WebsiteCeline George
Here we are going to discuss how to store data in Odoo 17 Website.
It includes defining a model with few fields in it. Add demo data into the model using data directory. Also using a controller, pass the values into the template while rendering it and display the values in the website.
Beginner's Guide to Bypassing Falco Container Runtime Security in Kubernetes ...anjaliinfosec
This presentation, crafted for the Kubernetes Village at BSides Bangalore 2024, delves into the essentials of bypassing Falco, a leading container runtime security solution in Kubernetes. Tailored for beginners, it covers fundamental concepts, practical techniques, and real-world examples to help you understand and navigate Falco's security mechanisms effectively. Ideal for developers, security professionals, and tech enthusiasts eager to enhance their expertise in Kubernetes security and container runtime defenses.
No, it's not a robot: prompt writing for investigative journalismPaul Bradshaw
How to use generative AI tools like ChatGPT and Gemini to generate story ideas for investigations, identify potential sources, and help with coding and writing.
A talk from the Centre for Investigative Journalism Summer School, July 2024
Slide Presentation from a Doctoral Virtual Open House presented on June 30, 2024 by staff and faculty of Capitol Technology University
Covers degrees offered, program details, tuition, financial aid and the application process.
Views in Odoo - Advanced Views - Pivot View in Odoo 17Celine George
In Odoo, the pivot view is a graphical representation of data that allows users to analyze and summarize large datasets quickly. It's a powerful tool for generating insights from your business data.
The pivot view in Odoo is a valuable tool for analyzing and summarizing large datasets, helping you gain insights into your business operations.
Still I Rise by Maya Angelou
-Table of Contents
● Questions to be Addressed
● Introduction
● About the Author
● Analysis
● Key Literary Devices Used in the Poem
1. Simile
2. Metaphor
3. Repetition
4. Rhetorical Question
5. Structure and Form
6. Imagery
7. Symbolism
● Conclusion
● References
-Questions to be Addressed
1. How does the meaning of the poem evolve as we progress through each stanza?
2. How do similes and metaphors enhance the imagery in "Still I Rise"?
3. What effect does the repetition of certain phrases have on the overall tone of the poem?
4. How does Maya Angelou use symbolism to convey her message of resilience and empowerment?
Split Shifts From Gantt View in the Odoo 17Celine George
Odoo allows users to split long shifts into multiple segments directly from the Gantt view.Each segment retains details of the original shift, such as employee assignment, start time, end time, and specific tasks or descriptions.
The Jewish Trinity : Sabbath,Shekinah and Sanctuary 4.pdfJackieSparrow3
we may assume that God created the cosmos to be his great temple, in which he rested after his creative work. Nevertheless, his special revelatory presence did not fill the entire earth yet, since it was his intention that his human vice-regent, whom he installed in the garden sanctuary, would extend worldwide the boundaries of that sanctuary and of God’s presence. Adam, of course, disobeyed this mandate, so that humanity no longer enjoyed God’s presence in the little localized garden. Consequently, the entire earth became infected with sin and idolatry in a way it had not been previously before the fall, while yet in its still imperfect newly created state. Therefore, the various expressions about God being unable to inhabit earthly structures are best understood, at least in part, by realizing that the old order and sanctuary have been tainted with sin and must be cleansed and recreated before God’s Shekinah presence, formerly limited to heaven and the holy of holies, can dwell universally throughout creation
Join educators from the US and worldwide at this year’s conference, themed “Strategies for Proficiency & Acquisition,” to learn from top experts in world language teaching.
Webinar Innovative assessments for SOcial Emotional SkillsEduSkills OECD
Presentations by Adriano Linzarini and Daniel Catarino da Silva of the OECD Rethinking Assessment of Social and Emotional Skills project from the OECD webinar "Innovations in measuring social and emotional skills and what AI will bring next" on 5 July 2024
Credit limit improvement system in odoo 17Celine George
In Odoo 17, confirmed and uninvoiced sales orders are now factored into a partner's total receivables. As a result, the credit limit warning system now considers this updated calculation, leading to more accurate and effective credit management.
How to Add Colour Kanban Records in Odoo 17 NotebookCeline George
In Odoo 17, you can enhance the visual appearance of your Kanban view by adding color-coded records using the Notebook feature. This allows you to categorize and distinguish between different types of records based on specific criteria. By adding colors, you can quickly identify and prioritize tasks or items, improving organization and efficiency within your workflow.
Lesson 11 - On Happiness. Introduction to Philosophy of a Human Personpptx
P7 lesson part three
1. P7 Physics ‘triple science’ Route map Over the next 24 lessons you will study: Friday 21 October 2011 P7.1 What is a telescope P7.2 Describing lenses P7.3 Refracting telescopes P7.4 Reflecting telescopes P7.5 Radio telescopes P7.7 Images of stars P7.8 The Sun, Moon and Earth P7.9 Observing the skies P7.10 Eclipses P7.11 Star distances P7.12 Star brightness P7.6 Ray diagrams P7.14 Galaxies-cepheid variable stars P7.15 Galaxies one or many P7.13 Star temperatures P7.16 Mapping the Milky Way P7.17 The changing Universe P7.18 Our Sun P7.19 The composition of stars P7.20 Emission spectra P7.21 Atoms and nuclei P7.22 Nuclear fusion P7.23 Behaviour of gases part one P7.24 Behaviour of gases part two P7.25 Types of stars P7.26 Structure of our Sun End of module test P7.27 Protostars P7.28 Star death
2. P7.13 Star temperatures Decide whether the following statements are true or false: Lesson objectives: Understand how star colour is related to its surface and core temperature. Understand how the spectrum of radiation (emitted colours) from hot objects depends on its temperature We will focus on. Friday 21 October 2011 First activity: List the factors that effect the luminosity of a star when we look at the night sky ? Think about a star's age, distance, content and mass. Literacy: Electromagnetic spectrum, spectrometer, peak frequency, frequencies, star brightness, starlight, distance, temperature, analysis, peak frequency, luminosity and colour. Numeracy: A hotter star will emit greater amounts of radiation at higher peak frequencies, for example it will emit more UV (ultra violet) light since UV light has a higher frequency than IR (infra red) light. PLTS Independent enquirers Creative thinkers Reflective learners We will focus on Team workers Effective participators Self managers
3. Extension questions: 1: Name some of the types of radiation in the electromagnetic spectrum and put them in order of increasing frequency ? 2: Give one use of a) infra red b) X-rays, c) Gamma waves and d) microwaves ? 3: Our star is a bright yellow colour. Estimate its surface temperature using the above information ? 4: Using the example of a filament light bulb explain how the filament changes colour as it gets hotter ? Know this: a: Know how the radiation given off by a star is linked to its surface temperature b: Know the different types of radiation in the electro-magnetic spectrum, for example UV, IR, X-rays and microwaves. Friday 21 October 2011 Introduction: Stars produce a constant stream of radiation which consists of a wide range of different frequencies. Most of the emitted radiation from stars is in the infrared (IR), visible and ultraviolet (UV) range of the electromagnetic spectrum. Not all stars are have the same appearance in the night sky. When you look carefully it can be seen that stars shine with different colours ranging from red to white. A star’s colour is dependant on the star’s surface temperature. A star with a red colour is at the cooler end with a surface tempearture of around 2000 o C. A star with a violet colour is at the hotter end with a surface temperature of 1500 o C. P7.13 Star temperatures
4. Key concepts Look at the photograph and information and answer all the questions: How does the a) frequency and b) the wave speed change from radio waves to gamma rays ? Explain what happens to the penetration ability as you move form radio waves to gamma waves ? Doctors exploit the penetrating ability of which wave to examine broken bones ? Electromagnetic waves are transverse waves which travel at a speed of 300,000 kms -1 through a vacuum. This is usually called the speed of light. All e.m waves transfer energy from one place to another and like visible light can be reflected by smooth, hard surface or refracted when they travel form one material to another. through transparent materials. The electromagnetic spectrum 10 -9 m 10 -6 m 10 -3 m 1 10 3 m 10 6 m 10 9 m Photon energy (J) Increasing energy and penetration Photons and the electromagnetic spectrum P7.13 a
5. Key concepts Look at the photograph and information and answer all the questions: Look at the picture above its shows the night sky which of course is actually one spiral arm of our own Galaxy the ‘Milky Way. Away form large cities and light pollution, you can see amazing array of different stars. The overall luminosity of a star will depend on its mass and distance from us. Its colour will depend on its surface temperature. The sun’s surface temperature is about 5000 °C what colour is it ? In the second picture which end of the colour spectrum would you find a hot star and which end would you find a colder star? 1000 °C 15000 °C 5000 °C P7.13 b Star temperatures
6. Key concepts Look at the photograph and information and answer all the questions: Billions of stars, found in millions of galaxies, but how do we identify groups of similar stars ? The new system reordered the classes into the order OBAFGKM where O stars are the hottest and each successive class is cooler with M being the coolest stars. Each letter was also divided into tenths of the range by adding a number 0-9 to the end. O stars are the least common and M are the most common found in the main sequence of stars. Look at the above diagram, estimate the surface temperature in o C of our own star, the sun ? Explain why larger or brighter stars often only last a few million years when compared to an average star like our own sun ? P7.13 c Star temperatures Type Colour Temp. Range % of stars Examples O Blue-violet >30,000 K 0.00003% Stars of Orion’s Belt B Blue-white 10,000 K - 30,000 K 0.13% Rigel A White 7,500 K - 10,000 K 0.6% Sirius F Yellow-white 6,000 K - 7,500 K 3% Polaris G Yellow 5,000 K - 6,000 K 7.6% Sun K Orange 3,500 K - 5000 K 12.1% Arcturus M Red-orange <3,500 K 76.5% Proxima Centauri
7. Key concepts P7.14 d Look at the photograph and information and answer all the questions: Looking at star brightness The area under the graph is an indication of star luminosity. The greater the area the hotter the star. At frequency X the two stars have different peak frequencies. The higher the peak at frequency X the hotter the star. The hotter the star the higher the peak frequency which means it has a higher proportion of radiation at higher frequencies. Look at the graph opposite left, which line on the graph show a hotter star? Which line on the graph shows data from a less luminous star ? Which line on the graph shows a star with a higher peak frequency ? Frequency Intensity of radiation hottest star coolest star UV light Infra red
8. P7.13 Plenary Lesson summary: Frequency violet surface colour Friday 21 October 2011 How Science Works: Research into the difference between our sun and a unique type of star which can vary both its luminosity and surface temperature called a ‘cepheid variable star.’ Preparing for the next lesson: The ________ of a star indicates how hot the _________ temperature is. The hotter the star the colour will be at the _________ end of the visible spectrum. On a graph of __________ against intensity a hotter star show higher peak frequency and luminosity (area under graph). Imagine living on Earth about 4.5 billion years into the future, you will see in the morning sky the sun turn red increasing rapidly in size. Eventually the red giant will increase and engulf even our planet instantly vapourise any surface life and water. What will be left will be a rocky planet devoid of any life and of course a cold planet without a sunrise or sunset . Decide whether the following statements are true or false : False True 3: Hotter stars tend to emit larger quantities of infra red radiation ? False True 2: A star’s luminosity is dependant on both its distance and size ? False True 1: Stars with a greater surface temperature will be red ?
9. P7.14 Galaxies – Cepheid variable stars Decide whether the following statements are true or false: Lesson objectives: Understand that some stars (cepheid variable stars) can vary both their brightness and surface temperature Understand the brightness- period relationship Understand how pulsing stars help scientists to measure astronomical distances. We will focus on. Friday 21 October 2011 First activity: Draw a graph that would show the diameter of a star expanding and contracting with time in a regulated way Draw both ‘Y’ and ‘X’ axis and place time for the ‘X’ axis and diameter on the ‘Y’ axis ? Literacy: Stars, luminosity, brightness, surface temperature, distance mass, size cepheid variable star, expansion, contraction, period, distance and galaxy. Numeracy: Our Sun is an average star which has a constant surface temperature, luminosity and colour. Variable stars (called Cepheid) can expand and contract in diameter by as much as 30% of their original size . PLTS Independent enquirers Creative thinkers Reflective learners We will focus on Team workers Effective participators Self managers
10. Extension questions: 1: Would a bright star have a higher or lower luminosity ? 2: Would a dim star have a higher or lower temperature ? 3: Would a dim star have a larger or small diameter ? 4: Why was it important that stars in the same galaxy are studied and compared when studying cepheid variable stars ? 5: Explain why astronomers are inserted in the distance between the milky way and other galaxies ? Know this: a: Know the relationship between brightness and period for Cepheid variable stars. b: Know how this relationship mean that we can calculate star distances. Friday 21 October 2011 Introduction: Most stars burn at a steady rate there are a few which don’t, they are called Cepheid variable stars. These stars, first seen in 1784, vary in brightness. Over a period of time they go from bright to dim and back again. These stars are actually expanding and contracting which then changes its luminosity and temperature. The diameter of these stars can change by up to 30%. Henrietta Leavitt studied these stars in nearby galaxies and saw a pattern between, the time it took to expand and contract back, and its luminosity. If you can calculate a star’s luminosity then you can then go on to calculate its distance from Earth. P7.14 Galaxies – cepheid variable stars
11. Key concepts P7.14 a Look at the photograph and information and answer all the questions: How long is the period of variation for the above star ? The graph shows a Cepheid variable star. The star gets dimmer and then returns to its original brightness. The length of time (called a single period) it takes to do this is important as this information can be used to calculate its luminosity. The time it take to go dim and then return to original brightness is called the period of variation . Time (days) Observed brightness A Cepheid variable star As a star’s luminosity varies over a single period, will its surface temperature also vary over the same time period ? 1 0 2 3 4 7 6 5
12. Key concepts P7.14 b Look at the photograph and information and answer all the questions: Explain what happens to the star’s size, luminosity and surface temperature over the seven day period ? Cepheid stars oscillate between two states: In one state, the star is compact and large temperature and pressure gradients build up in the star. These large pressures cause the star to expand. When the star is in its expanded state, there is a much weaker pressure gradient. Without the pressure gradient to support the star against gravity, the star contracts and the star returns to its compressed state (see the above diagram) Time (days) brightness A Cepheid variable star Another star has a period of variation of 10 days, which star will have the highest luminosity on day 5 ? star diameter 1 0 2 3 4 7 6 5
13. Key concepts P7.14 c Look at the photograph and information and answer all the questions: Look at the four pictures taken on May 4 th to May 20 th when its this start at its large by diameter and smallest by diameter ? The four pictures above shows a Cepheid variable star. The star can be seen brightly on may 4 th but gets dimmer for a week and then returns to original brightness by may 20 th . Without the presence in the galaxies across the Universe of these Cepheid stars Hubble would not have been able to calculate the distances to other galaxies. How many days does this star take to do a variation cycle ? A Cepheid variable star May 4 th May 9 th May 16 th May 20 th
14. Key concepts P7.14 d Look at the photograph and information and answer all the questions: luminosity time period A D B C Place the four stars A-D into order with the brightest star first ? Why can star A have a greater luminosity than star B even though its smaller and less bright ? Luminosity versus time in a Cepheid star Star brightness can be easily seen and measured if the period of variation is also known then the luminosity can be calculated. Brightness of stars are assigned a number starting with the brightest star starting at about -1 magnitude. Dimmer stars are zero or positive numbers. The larger the number means the dimmer the star is. For example, a star -1 magnitude is brighter than a star 0 magnitude. A star 0 magnitude is brighter than a star 1 magnitude and so on Magnitude sequence for stars starting with the brightest is -1, 0, 1, 2, 3, 4, 5, 6, 7, 8, 9, 10 magnitude, ... etc Looking at star brightness
15. P7.14 Plenary Lesson summary: period cepheid expands rate Friday 21 October 2011 Most stars are currently classified using the letters O , B , A , F , G , K and M (usually memorized by astrophysicists as "O be a fine girl, kiss me"), where O stars are the hottest and the letter sequence indicates successively cooler stars up to the coolest M class. According to an informal tradition, O stars are "blue", B "blue-white", A stars "white", F stars "yellow-white", G stars "yellow", K stars "orange", and M stars "red.” How Science Works: Research into the current view of the Universe as a collection of billions of galaxies in constant expansion and look at the work of Harlow Shapely and Edwin Hubble. Preparing for the next lesson: There is a small group of stars that burn at a varying ______. These stars are called ______ variable stars, their diameter _________ and contracts over a certain ______ of time. This is the period of variation the longer this period is the more luminous the star. Decide whether the following statements are true or false : False True 3: In the contracted phase of a star its at its brightest ? False True 2: In the expanded phase of a star is at its dimmest ? False True 1: luminosity is linked to star temperature ?
16. P7.15 Galaxies – one or many Decide whether the following statements are true or false: Lesson objectives: Understand that the Universe is a collection of billions of galaxies each containing many billions of stars. Understand how both Harlow Shapley's and Edwin Hubble’s work has effected our picture of the galaxies We will focus on. Friday 21 October 2011 First activity: In 1923, the work of Edwin Hubble’s work on the Andromeda Galaxy finally showed the World that there were other Galaxies outside our own Milky Way. Explain this was one of the most improtant breakthrough in modern science ? Literacy: Galaxies, stars, universe, clusters, telescopes, galaxies, astronomer, nebulae, milky way, and globular clusters. Numeracy: There are between 200 - 400 billion stars in our galaxy, the Milky Way. There are possibly 100 billion galaxies, this gives approximately 3 x 10 24 stars in the Universe. So about 3 septillion stars altogether...amazing !! PLTS Independent enquirers Creative thinkers Reflective learners We will focus on Team workers Effective participators Self managers
17. Extension questions: 1: Prior to the work of Harlow Shapley, scientists thought that the milky way was at the very centre of the Universe, explain why scientists might have wrongly first thought this ? 2: How did Harlow Shapley’s work begin to change this view ? 3: How did Curtis Heber’s work further improve our view of galaxies and the Universe ? 4: What pieces of information would Edwin Hubble have needed to know to work out the star distance ? Know this: a: Know that the ‘Universe’ is a collection of billions of Galaxies like our own Milky Way. b: Know how Shapley’s and Hubble's work have helped us understand and improve the work of the previous scientists. Friday 21 October 2011 Introduction: The field of atronmony and the use of telscopes has been crucial in building up a picture of what the universe actually looks like. Telescopes revealed fuzzy objects that were bigger than individual stars, they named them nebulae. Harlow Shapley measured the distances of nebulae and found that they were clusters of stars ourside our own milk way. He called them globula clusters. Curtis Heber then demonstrated that these globular clusters were very far away and were actually galaxies in their own right and didn’t orbit the Milky Way. In 1923 the matter was decided using the results from Edwin Hubble he spotted a cepheid variable star and when he measured it it turned out to be millions of light years away far greater than the dimensions of the Milky way. Hubble showed that Andromeda Nebula was a giant galaxies containing billions of stars outside of our own galaxy. P7.15 Galaxies – one or many
18. Key concepts P7.15 a Look at the photograph and information and answer all the questions: Explain why this single picture taken over 10 days in 1998 has radically change the way we view our own Universe ? It is estimated that some of the galaxies picture above are up to 13 billion light years away. Explain why if life does exist there we may never know of its existance ? The Hubble telescope launched in 1996 by the shuttle program is in a fixed orbit outside the Earth’s atmosphere. Over the Christmas holidays in 1998 its camera was pointed at an area of space with no visible stars for 10 days. When the picture was sent to Earth it showed that this small part of deep space was full of galaxies. Each speck on the picture left is a galaxy contain up to 100 billion stars Hubble ‘deep space photograph in 1998
19. Assessment for learning...key concepts P7.15 a Look at the photograph and information and answer all the questions: Explain why the most common element found in the Eagle nebula is hydrogen gas which is the building material for all stars ? Explain why larger or brighter stars often only last a few million years when compared to an average star like our own Sun ? Billions of stars, found in millions of galaxies, filling billions of light years of space, but how are galaxies and stars formed. In 1998, the Hubble telescope and one of its many images, finally gave us spectacular evidence that tells scientists how stars and galaxies are formed. The Eagle nebula (pictured below) is a cloud of hydrogen and dust millions of light years across. At the end of each finger like protrusion, the gravitational forces form a ball of hydrogen. Huge gravitational forces superheat the hydrogen so that nuclear fusion begins, light is produced and a star is born.
20. P7.15 Plenary Lesson summary: disproved development telescope galaxies Friday 21 October 2011 In 1915 Harlow Shapley used Cepheids to place initial constraints on the size and shape of the Milky Way, and of the placement of our Sun within it. In 1924 Edwin Hubble discovered Cepheid variables in the Andromeda galaxy. That settled the debate, of whether the Milky Way was one of many galaxies that constitutes the Universe. How Science Works: Research into the nature of our own Galaxy, the Milk Way Preparing for the next lesson: The work of Shapley, Hubble and Curtis has been crucial in our understanding of the _________. They showed a clear _________ of theories until arriving at one which has not been _________. Hubble's work with Cepheid's and Andromeda was so important that they named a ___________ after him. Decide whether the following statements are true or false : False True 3: Shapley's work on nebulae turned out not to be correct ? False True 2: Hubble used Cepheid stars to calculate the brightness of different stars ? False True 1: Edwin Hubble designed the Hubble Space Telescope ?
21. P7.16 Mapping the Milky way Decide whether the following statements are true or false: Lesson objectives: Understand that the ‘Milky Way’ is just one of many billions of Galaxies known to exist in the Universe Understand that knowledge of our own Milky Way help us scientists understand how the Universe is built We will focus on. Friday 21 October 2011 First activity: We are (solar system) located midway on just pone of the five spiral arms that make up the milky way galaxy. It takes light about 100,000 years to travel from one end to the other end of our own galaxy. The Andromeda Galaxy is a staggering 2 million light years away form us. If we sent a question to intelligent life at the speed of light to a star in the Andromeda Galaxy, how long would we have to wait for an answer ? Literacy: Galaxies, stars, universe, clusters, telescopes, galaxies, astronomer, nebulae, milky way, and globular clusters. Numeracy: The Milky Way is where our own solar system is located in one of its spiral arms. It is a typical galaxies from about 4.5 billion years old formed form hydrogen and other cosmic build blocks !! PLTS Independent enquirers Creative thinkers Reflective learners We will focus on Team workers Effective participators Self managers
22. Extension questions: 1: Explain why we will never have a true picture of the Milky Way ? 2: Name one star constellation found in the night sky ? 3: Galaxies are formed by massive clouds of dust and gases in space: a) What’s the force that attracts the clouds of dust and hydrogen gas together to form stars. b) Once formed, the star has a stable life for billions of years. 4: Describe the two main forces at work in the star during this period. c) What happens to the star once this stable period is over ? Know this: a: Know that the ‘Milky Way’ is just one of billions of galaxies that form our Universe. b: Know how Shapley’s and Hubble's work have helped us understand and improve the work of the previous scientists. Friday 21 October 2011 Introduction: Look up at the night sky and you are looking through a very small part of our own galaxy the Milky Way. Although light pollution in cities hinders our view of the sky at night, far away in the unpopulated countryside the Milky Way is awesome. Viewed at night you can see why it is named the Milky Way. A milky light crosses the sky, full of stars, all many hundreds of light years away. Our own galaxy stretches over 100,000 light years across. Our night sky moves around the pole star (named Polaris) P7.16 Mapping the Milky way
23. Key concepts P7.16 a Look at the photograph and information and answer all the questions: The Milky Way Galaxy, is the galaxy in which the Solar System is located. The Milky Way is a barred spiral galaxy that is part of the Local Group of galaxies. It is one of billions of galaxies in the observable universe. Some sources hold that, strictly speaking, the term Milky Way should refer exclusively to the band of light that the galaxy forms in the night sky, while the galaxy should receive the full name Milky Way Galaxy, or alternatively the Galaxy Explain why the two picture opposite are an artists impression rather than a real photograph ? Explain why most of the the mass of a galaxy (stars) is found towards its centre ? An average galaxy has about 100 billion stars, explain why life elsewhere is almost certain to exist but we may never know that it does ? The milky way
24. Key concepts P7.16 a Look at the photograph and information and answer all the questions: Explain why you cannot see the full beauty of the Milky Way in a city like London ? Why can the Polaris star been used to navigate at night ? A collection of stars, this five armed spiral galaxy is home to our Sun and its nine planets. Our own galaxy is vast, over 100,000 light year across. In cities and other populated areas we can only see a few stars because of light pollution. Time lapse photography shows us that the night sky revolves around a central star called Polaris. This star is used to navigate north because its position remains unchanged throughout the night. The Milky Way
25. P7.16 Plenary Lesson summary: centre spiral way years Friday 21 October 2011 Our own galaxy is vast, over 100,000 light year across. In cities and other populated areas we can only see a few stars because of light pollution. It is worth just once in your life to go to the rote countryside and see the full beauty of the Milky Way ! How Science Works: Research into how our Universe is expanding and Hubble constant Preparing for the next lesson: The Milky _____ is a five _______ Galaxy spanning just over 100,000 light _______ across. It is home to our solar system and of course planet Earth. The majority of the Milky way’s mass is found towards its _______. Decide whether the following statements are true or false : False True 3: The Sun is a the very centre of the Milky Way ? False True 2: It takes light 10,000 years to travel across the entire width of the Milky Way ? False True 1: The Milky Way is a four spiral Galaxy ?
26. P7.17 The changing Universe Decide whether the following statements are true or false: Lesson objectives: Understand the evidence for the current view that the Universe is in constant expansion or recession. Understand Hubble’s constant and a Galaxy's red shift We will focus on. Friday 21 October 2011 First activity: If the Universe started with a big bang form a single point in space explain why galaxies continue to move away form one another ? Literacy: Expansion, recession, galaxy, telescope, nebula, Cepheid variables. Numeracy: Speed of = Hubble X distance Recession constant The Hubble constant = 72 ±8 km/s per MPC PLTS Independent enquirers Creative thinkers Reflective learners We will focus on Team workers Effective participators Self managers
27. Extension questions: 1: What technology enabled Hubble to do his work ? 2: Why had other previous scientists been unable to do see work ? 3: How does the big bang theory of the Universe account for its creation and outline the evidence which supports the big bang theory ? 4: What is meant by the term ‘red shift’ as used in astronomy and explain how the red shift helps us to find out more about our own Universe ? Know this: a: Know the evidence for the current view that the Universe is in constant expansion. b: Know about Hubble’s constant and the red shift. Friday 21 October 2011 Introduction: Hubble used the largest telescopes available to him (reflectors of 5m). He decided a previously unknown phenomenon that the galaxies all seem to be receeding (moving away) from us. He looked at spectra of stars and saw that light was shifted to the red end – the red shift. Hubble saw that the further away the galaxy the faster it was receeding this led to 2 very important ideas The Universe is expanding so was probably smaller in the past The Universe probably started out by exploding from a single point – big bang theory P7.17 The changing Universe
28. Key concepts P7.17 a Look at the photograph and information and answer all the questions: What is the speed of recession when the distance is 20 mpc and the Hubble constant is 70 km/s per mpc? What are the units of all the term in the equation? Hubble used the early work of Leavitt to determine the distance of at least 10 galaxies. He also made another great discovering that all galaxies were moving away from. This produced a red shift which occurs when a light source is moving away. If galaxies were moving towards us a blue shift would happen. The Hubble constant took many years to find an accurate value but its now taken to be 72 ±8 km/s per MPC. Speed of = Hubble X distance Recession constant Distance (mpc) speed of recession (km/s) 10 6 2x10 6 1000 500 X X X X X X X The Hubble constant
29. Look at the photograph and information and answer all the questions: If all observable planets acquired a blue shift instead of a red shift what would this mean would be happening ? Explain why scientists cannot yet answer the question ‘will the Universe contract from its current size ? Since the ‘big bang’ the Universe continues to expand, but what other evidence do we have to support the big bang theory proposed by Stephen Hawking. If we observe the many thousands of visible galaxies using the Hubble telescope, they all have a red shift meaning that they are always moving away from us. These images proves that the Universe and its galaxies are in constant expansion. (If the galaxies has a blue shift they would be in contraction or moving towards us) Big bang the expanding Universe Key concepts P7.17 b Expansion Contraction Red shift Blue shift
30. Look at the photograph and information and answer all the questions: Why did Ptolemy and his peers in 140 AD think that the Earth was at the centre of the Universe ? Hubble's observation that the Milky Way was just one of many millions of galaxies was an important discovery…explain why ? Humans, for thousands of years have asked questions about their own history, the history of the solar system and Universe. Early philosophers and modern scientists have given us different answers to the one single question: How and when did the Universe begin ? Over the last two thousand years, many different theories have been offered by scientists to explain what events began, that led to the formation of the Universe and all the galaxies that we observe today . Ptolemy: Proposes in 140 AD that the Earth is a sphere and is at the very centre of the Universe. Copernicus: Proposes in 1600 AD that the Sun is the very centre of the Universe, with the Earth orbiting it. Hubble: Proposes that our galaxy, the Milky Way is just one of billions of similar Galaxies. Hawkins: Popularised that the Universe started with a big bang around 14 billion years ago and is still in constant expansion. Key concepts P7.17 c
31. P7.17 Plenary Lesson summary: red shift receding spectra Hubble Friday 21 October 2011 Hubble went on to discover many more stars in other nebulas located outside the Milky Way. Whilst studying these other galaxies he found that they contained many similar features of our own Milky Way Galaxy. He found they contained stars called novas that suddenly flair brightly and globular cluster, compact groups of stars. Hubble finally proposed his theory that nebulas where actually other galaxies much like our own. How Science Works: Research the composition of stars and the anatomy of our own star, the Sun Preparing for the next lesson: __________discovered that the universe is ___________ (moving apart). He did this by proving that the light given off by stars shifts over time to the red end of the visible _____ this is called the ______________ Decide whether the following statements are true or false : False True 3: Hubble's initial constant of 500km/s per mpc was correct ? False True 2: There’s a linear relationship between a star’s distance and speed of recession ? False True 1: 10 7 parsec = 1 megaparsec ?
32. P7.18 Our Sun Decide whether the following statements are true or false: Lesson objectives: Understand the composition and anatomy of stars like our own sun. Understand the life cycle of our own star the Sun. We will focus on. Friday 21 October 2011 First activity: Explain why in about 4.5 billion years, life will stop, all life will stop on planet Earth ? Literacy: Stars, anatomy, surface, surface temperature core, convection currents, light, absorption, emission, spectrum, composition, atmosphere, sunlight and prism. Numeracy: The Sun is currently half way through its 9 billion year life cycle. It is currently consuming about 300,000 tones of hydrogen every second...fear not it has sufficient reserves of hydrogen for another 4.5 billion years . PLTS Independent enquirers Creative thinkers Reflective learners We will focus on Team workers Effective participators Self managers
33. Extension questions: 1: Explain what stars like the sun are formed from ? 2: What’s the force that attracts the clouds of dust and hydrogen gas together to form stars. 3: Give two forms of energy that is emitted by the Sun ? 4: What type of radiation can increase the risk of skin cancer ? 5: Why should you never look at the Sun directly or through telescope ? Know this: a: Know the composition and anatomy of stars like our sun. b: Know the life cycle of the Sun over its 9 billion year life. Friday 21 October 2011 Introduction: The Sun is the closest star to Earth and represents 99.1% of the mass of the entire solar system. The Sun formed over four and a half billion years ago, but it will keep shining for at least another five billion years. The Sun’s surface is called the photosphere. The temperature of the photosphere is about 6,000 centigrade. Its core is under its atmosphere. The temperature at the core, or very middle, of the Sun, is about 27 million centigrade. The Sun is 109 times wider than Earth, and is 333,000 times heavier. That means if you put the Sun on a scale, you would need 333,000 objects that weigh as much as the Earth on the other side to make it balance. . P7.18 Our Sun
34. Key concepts P7.18 a Look at the photograph and information and answer all the questions: Name three types of radiation emitted by the Sun ? Although all electromagnetic waves travel through space from the Sun to Earth’s surface, sound doesn’t. Explain why this is a good thing ? The Sun is the star at the centre of the Solar System. It has a diameter of about 1,392,000 km, about 109 times that of Earth, and its mass is 330,000 times that of Earth. About three quarters of the Sun's mass consists of hydrogen, while the rest is mostly helium. Less than 2% consists of heavier elements, including oxygen, carbon and neon.
35. Look at the photograph and information and answer all the questions: Anatomy of the Sun Explain why the temperature cools as you move from the core of the Sun to its surface ? What element is the Sun made from and how could prove your answer ? The sun is made up of several layers, each layer has unique properties, which are vital to the sun's functions. The centre of the sun, the Core, is the only part of the sun that actually makes energy. The temperature in the Core is about 15,000,000 o C. The next layer of the sun is the Radioactive Zone, , the temperature here is about 5,000,000 o C. The layer that is next is called the Convection Zone, where solar material rises and falls due to heating and cooling. The temperature here reaches only 5,800 o C. The next section of the sun is called the Photosphere, which is actually what you see when you look at the sun. Key concepts P7.18 b
36. Look at the photograph and information and answer all the questions: Scientists believe that in the early Universe only hydrogen existed. Explain how other elements have formed ? Explain why and how all life will eventually end here on planet Earth ? The Sun has a lifespan of about 9 billion years and is already halfway through its life using up to 300,000 tonnes of hydrogen gas every second. Eventually, when all the hydrogen and helium is consumed, the Sun will rapidly expand forming a red giant that engulfs and scorches the first four planets including Earth. What follows then is its contraction, the formation of a white dwarf and then a neutron star. During this phase heavier elements are formed. The life cycle of an average star like our sun Stellar nebula Average star Red Giant Planetary nebula White Dwarf Neutron star 4.5 billion years B.C 4.5 billion years A.D 4.6 billion years A.D Key concepts P7.18 c Life cycle of an average star
37. P7.18 Plenary Lesson summary: core surface life heat Friday 21 October 2011 The mean distance of the Sun from the Earth is approximately 149.6 million kilometres, though the distance varies as the Earth moves from perihelion in January to aphelion in July. At this average distance, light travels from the Sun to Earth in about 8 minutes and 19 seconds. This means we never actually see the Sun where it is just where it was 8 mins and 19 seconds ago. How Science Works: Research into how we can determine the composition of stars like the Sun. Preparing for the next lesson: The Sun gives off ______ and light that the Earth needs to support _______.. The ____________ temperature of the Sun is about 6000 o C. The Sun is made out of 92% hydrogen, 7% helium and the rest is other low number gasses? The Sun’s ______ is the hottest part of its matter. Decide whether the following statements are true or false : False True 3: The Sun is half way through its life cycle ? False True 2: The gravitational pull of the Sun keeps Earth in its orbit? False True 1: The Sun is largely composed of chlorine and oxygen gases ?
38. P7.19 The composition of stars Decide whether the following statements are true or false: Lesson objectives: Understand the composition and anatomy of stars like our own sun. Understand what absorption and emission spectra and how these spectra are used to determine star composition We will focus on. Friday 21 October 2011 First activity: Explain how by analysing the light emitted from our own star the Sun can help build up a picture of the elements that make up its composition ? Literacy: Stars, anatomy, surface, surface temperature core, convection currents, light, absorption, emission, spectrum, composition, atmosphere, sunlight and prism. Numeracy: The visible range of the electromagnetic spectrum has wavelengths of between 390 – 750 nm . Red light is at the 750nm end and violet light is at the 390nm end of the spectrum. PLTS Independent enquirers Creative thinkers Reflective learners We will focus on Team workers Effective participators Self managers
39. Extension questions: 1: Name, in order, the colours of light in the visible part of the electromagnetic spectrum ? 2: Draw a diagram to show how a prism works ? 3: What's the difference between a emission and a absorption spectrum ? 4: What elements are present in the Earth’s atmosphere ? 5: What elements are present in the Sun’s atmosphere ? Know this: a: Know the composition and anatomy of stars like our Sun. b: Know what absorption and emission spectra show and how we have determined star composition. Friday 21 October 2011 Introduction: The light given out by a star can be analyzed using a prism to split the light up. When this was performed with sunlight in 1802 the resulting emission spectra showed black lines which means that some wavelengths were missing. These line are called Fraunhofer lines. These missing sections were analyzed closer and eventually it was discovered that certain elements in the stars atmosphere absorb certain wavelengths of light resulting in the fraunhofer lines. Each element will give a unique absorption spectrum by absorbing different parts of the visible light. Then were able to tell what was present in the stars atmosphere by analyzing the emission spectrum. P7.19 The composition of stars
40. Key concepts P7.19 a Look at the photograph and information and answer all the questions: What are the black bands of missing wavelengths called ? Explain why the emission spectra form deep space is different to the emission spectra of our own Sun ? When elements like sodium and magnesium burn with oxygen they give out light at certain colour or wavelengths. The spectrum form our own Sun and deep space are of course very different. The spectrum of sunlight above shows black band, these correspond to areas where elements in the suns atmosphere have absorbed these specific wavelengths. Light emission Our Sun Deep space Light spectrum from our Sun Light spectrum from deep space prism prism
41. Key concepts P7.19 b Look at the photograph and information and answer all the questions: Compare the emission spectra of our sun and hydrogen ? Explain why we know the Sun contains other elements in addition to hydrogen ? When the electrons in the atom are excited, (heated) the extra energy pushes the electrons to higher energy orbits. When the electrons fall back down and leave the excited state, energy is re-emitted in the form of a photon. The wavelength of the photon is determined by the difference in energy between the two states. These emitted photons form the element's emission spectrum . Light emission Our Sun Hydrogen Light spectrum from our Sun Light spectrum of hydrogen prism prism H 1 1
42. P7.19 Plenary Lesson summary: elements spectra lower stars Friday 21 October 2011 The Sun’s emission spectrum gives scientists a picture of the composition of the Sun,. Far form being simple it is very complex but it does give evidence that the Sun contains elements like hydrogen, helium and oxygen. How Science Works: Research into understand emission spectra and how atoms of different elements emit light by emitting photons with discreet energy levels. Preparing for the next lesson: Emission ______ can be used to determine to composition or ______ present in __ like our own Sun and even in deep space. Each element will give a unique emission spectra due to photons jumping form higher to ______ energy levels. Decide whether the following statements are true or false : False True 3: If a photon has been absorbed the resulting spectra will have an area of black ? False True 2: The emission spectra of hydrogen is different to the emission spectra of helium ? False True 1: In deep space, there is very little light emitted ?
43. P7.20 Emission spectra Decide whether the following statements are true or false: Lesson objectives: Understand why different elements have different emission spectra Understand that when electrons drop from one energy level to the next it emits a single photon of light or packet of energy. We will focus on. Friday 21 October 2011 First activity: Can you remember the flame test for metallic elements like sodium and copper. The following five metals all give distinctive coloured flames when burnt in a Bunsen burner on a blue flame, give their colours a) Sodium b) Potassium c) Copper d) Magnesium and e) Lithium ? Literacy: Emission spectra, excited, energy levels, photon, emit, absorb, electron and energy levels. Numeracy: Electrons inside an atom can only have certain values of energy. Electrons can jump or fall form one energy level to the next. As these lose energy, they can emit the energy as a single photon which is a packet of energy PLTS Independent enquirers Creative thinkers Reflective learners We will focus on Team workers Effective participators Self managers
44. Extension questions: 1: Define the term photon ? 2: Will light be emitted or absorbed if an electron jumps up an energy level ? 3: Will light be emitted or absorbed if an electron drop an energy level ? 4: Draw a diagram to represent absorption of light by an electron ? 5: Draw a diagram to represent emission of light by an electron ? Know this: a: Know why different elements have different absorption spectra b. Know that when an electrons drops from one energy to the next it emits a single photon (packet of energy) Friday 21 October 2011 Introduction: The absorption spectra of each element is unique. This is because all elements emit light in a different way. Light is emitted by an element when its electrons lose energy, as its lost in form of light energy. Light can also be absorbed by an atom. Electrons have certain set values of energy, if an electron drops to a lower energy level it emits a package of light called a photon. If an elecron jumps up an energy level it absorbs a photon of light and the resulting spectrum will show missing wavelengths of light. P7.20 Emission spectra
45. Key concepts P7.20 a Look at the photograph and information and answer all the questions: Albert Einstein developed the theory that radiation including waves belonging to the electromagnetic spectrum is always emitted and absorbed as packets of energy called photons. He stated that the total amount of energy transfer for a beam of radiation can be calculated by taking into account: the energy of each photon the number of photons arriving each second on the absorbers surface Look at the two cars opposite, they are identical except their colour. Explain which one will heat up the most on a hot summer’s day ? If both are bathed in the same sunlight explain your answer to the first question in terms of photons and how they are absorbed onto the car’s surface ? photons photons
46. Assessment for learning...key concepts P7.20 b Look at the photograph and information and answer all the questions: Look at the emission spectra for a) hydrogen and b) helium what are the strongest colour and do you see these colours in spectra from the Sun ? Explain clearly why Fraunhofer lines (black line in the first spectra) are present on the emission spectrum of sunlight. ? If you analyse light from our sun (the solar spectrum) apart from some colours that are absorb by the Sun’s own atmosphere, you see a full spectrum of colours from red with a wavelength of 700 nm to violet with wavelength of about 400 nm. If you analyse light from pure elements like hydrogen, lithium, helium and sodium, you will set distinct emission spectra. By comparing the two you can begin to build a picture of the elements present as part of the Sun’s huge mass. Emission spectra and photons Sun’s emission spectra Hydrogen’s emission spectra Helium’s emission spectra Mercury’s emission spectra Uranium’s emission spectra
47. Key concepts P7.20 c Look at the photograph and information and answer all the questions: What would happen if the electron from the middle energy level jumped up to the upper energy level ? If the energy gap between energy levels is large would the photon emitted be high or low frequency ? Therefore, would it be a short or long wavelength ? In this simplified diagram above right three different energy levels are shown. Electrons can jump between these energy levels. The electron illustrated in green drops from the middle energy level to the lowest energy level. When this happens a photon of light is emitted. The energy of the photon is equal to the difference in the energy levels. = electron Emission spectra and photons Photon emitted Increasing energy
48. Key concepts P7.20 d Look at the photograph and information and answer all the questions: If an atom emitted mainly red light would it be emitting low or high energy photons ? Explain the link between the energy status of a photon and its wavelength ? In this simplified diagram above two electrons are shown. The electron shown in blue jumps form the highest to the middle energy level releasing a smaller amount of energy as a photon. The second electron shown in green jumps form the middle to lowest energy level. Here the jump is larger therefore the photon has more energy and a shorter wavelength. Photon emitted (high energy short wavelength) Increasing energy Photon emitted (low energy long wavelength) Colour of light from a high energy photons (blue) Colour of light from a low energy photons (red) Emission spectra and photons
49. P7.20 Plenary Lesson summary: absorb emits photon energy Friday 21 October 2011 In 1913, it was Neils Bohr who proposed that electrons revolves around the atom’s nucleus with a definite fixed energy, without emitting or absorbing energy. These energy levels are called Principal Quantum Levels. Level n = 1 is closest to the nucleus of the atom and of lowest energy. How Science Works: Research in atoms and their nuclei and the sub atomic particles know as electrons, protons and neutron. Also find out about the work of Geiger, Marsden and Rutherford. Preparing for the next lesson: If an electron drops an energy level it _______ a photon, which is a packet of _______ . If an electron jumps to a higher energy level it will ______ a photon. The amount of energy absorbed or emitted is calculated by the difference between the two energy levels. Decide whether the following statements are true or false : False True 3: If a photon has been absorbed the resulting spectra will have an area of black ? False True 2: Photons are packets of sound energy ? False True 1: Electrons can be made to move into higher and lower energy levels ?